An updated measurement of the Hubble constant from near-infrared observations of Type Ia supernovae^⋆

¹ Institute of Space Sciences (ICE, CSIC), Campus UAB, Carrer de Can Magrans, s/n, 08193 Barcelona, Spain
e-mail: lgalbany@ice.csic.es
² Institut d’Estudis Espacials de Catalunya (IEEC), 08034 Barcelona, Spain
³ Institute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu, HI 96822, USA
⁴ Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA
⁵ Department of Physics and Astronomy, Johns Hopkins University, Baltimore, MD 21218, USA
⁶ Institute of Astronomy and Kavli Institute for Cosmology, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK
⁷ Department of Physics and Astronomy, Aarhus University, Ny Munkegade 120, 8000 Aarhus C, Denmark
⁸ European Southern Observatory, Karl-Schwarzschild-Strasse 2, 85748 Garching, Germany
⁹ Observatories of the Carnegie Institution for Science, 813 Santa Barbara St., Pasadena, CA 91101, USA
¹⁰ Department of Physics, Duke University, Durham, NC 27708, USA
¹¹ The Oskar Klein Centre for Cosmoparticle Physics, Department of Physics, Stockholm University, 10691 Stockholm, Sweden
¹² School of Physics, Trinity College Dublin, College Green, Dublin 2, Ireland
¹³ Department of Physics and Astronomy, Rutgers the State University of New Jersey, 136 Frelinghuysen Road, Piscataway, NJ 08854, USA

Received: 5 September 2022
Accepted: 15 September 2023

Abstract

We present a measurement of the Hubble constant (H₀) using type Ia supernovae (SNe Ia) in the near-infrared (NIR) from the recently updated sample of SNe Ia in nearby galaxies with distances measured via Cepheid period-luminosity relations by the SH0ES project. We collected public near-infrared photometry of up to 19 calibrator SNe Ia and 57 SNe Ia in the Hubble flow (z > 0.01), and directly measured their peak magnitudes in the J- and H-band by Gaussian processes and spline interpolation. Calibrator peak magnitudes together with Cepheid-based distances were used to estimate the average absolute magnitude in each band, while Hubble-flow SNe were used to constrain the zero-point intercept of the magnitude–redshift relation. Our baseline result of H₀ is 72.3 ± 1.4 (stat) ±1.4 (syst) km s⁻¹ Mpc⁻¹ in the J-band and 72.3 ± 1.3 (stat) ±1.4 (syst) km s⁻¹ Mpc⁻¹ in the H-band, where the systematic uncertainties include the standard deviation of up to 21 variations of the analysis, the 0.7% distance scale systematic from SH0ES Cepheid anchors, a photometric zero-point systematic, and a cosmic variance systematic. Our final measurement represents a measurement with a precision of 2.8% in both bands. Among all the analysis variants, the largest change in H₀ comes from limiting the sample to those SNe from the CSP and CfA programs; they are noteworthy because they are the best calibrated, yielding H₀ ∼ 75 km s⁻¹ Mpc⁻¹ in both bands. We explore applying stretch and reddening corrections to standardize SN Ia NIR peak magnitudes, and we demonstrate that they are still useful to reduce the absolute magnitude scatter and, which improves its standardization, at least up to the H-band. Based on our results, in order to improve the precision of the H₀ measurement with SNe Ia in the NIR in the future, we would need to increase the number of calibrator SNe Ia, to be able to extend the Hubble–Lemaître diagram to higher redshift, and to include standardization procedures to help reduce the NIR intrinsic scatter.